in Modelling of Stellar Atmospheres

By Bernd Freytag, S. Hofner, Enid L. Livingston. 2004

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Citations in the corpus

Evolutionary state of magnetic chemically peculiar stars (2006, background): “However, it not yet clear (observationally nor theoretically) if and how these fields evolve during the main sequence phase.”
Pre-main-sequence isochrones - II. Revising star and planet formation time-scales (2013, methodology): “The atmospheric models used are the same as those in Paper I and consist of PHOENIX BT-Settl models (Allard, Homeier & Freytag 2011)2 for 400 ≤ Teff ≤ 7800 K and the Kurucz ATLAS9/ODFnew models (Castelli & Kurucz 2004)3 for 8000 ≤ Teff ≤ 50 000 K.”
FUNDAMENTAL PROPERTIES OF STARS USING ASTEROSEISMOLOGY FROM KEPLER AND CoRoT AND INTERFEROMETRY FROM THE CHARA ARRAY (2012, methodology): “To further test these results, we have used an independent method to determine bolometric fluxes for four stars by combining publicly available flux-calibrated ELODIE spectra (Prugniel et al. 2007), broadband photometry and ATLAS9 models (Castelli & Kurucz 2003, 2004).”
The Second APOKASC Catalog: The Empirical Approach (2018, methodology): “The luminosity is then transformed into absolute magnitudes in several filters using bolometric corrections inferred from the library of ATLAS 9 synthetic spectra from Castelli & Kurucz (2003) at the spectroscopic Teff and metallicity and the asteroseismic surface gravity.”
On the age of the β Pictoris moving group (2014, methodology): “The isochrones have been transformed into the observational plane using the atlas9 atmospheric models of Castelli & Kurucz (2004), for which we assume no α-element enhancement.”
Transforming observational data and theoretical isochrones into the ACS/WFC Vega-mag system (2004, methodology): “We computed ACS colour indices by using the homogeneous set of ODFNEW model atmospheres and synthetic fluxes7 (Castelli & Kurucz 2003) computed with the Kurucz ATLAS9 code.”
Evolution of asymptotic giant branch stars. II. Optical to far-infrared isochrones with improved TP- (2007, methodology): “Moreover, the library has been extended with the Loidl et al. (2001) synthetic C-star spectra for 3600 >∼ (Teff/K) >∼ 2600, derived from hydrostatic model atmospheres computed with MARCS (see also Höfner et al. 2003, for more details).”
Improving PARSEC models for very low mass stars (2014, methodology): “These tables of BCλ will be used later in this paper, for the Teff interval between 2600 and 6000 K, as an alternative to the previous tables used in PARSEC – which were based on Castelli & Kurucz (2003) and Allard et al. (2000) model atmospheres.”
New PARSEC evolutionary tracks of massive stars at low metallicity: testing canonical stellar evolution in nearby star-forming dwarf galaxies (2014, methodology): “In the ranges of effective temperature, surface gravity, and metallicity relevant to this work, we use the spectra derived from the ATLAS9 model atmospheres (Castelli & Kurucz 2003), which are well calibrated against observations.”
Accurate fundamental parameters for lower main‐sequence stars (2006, methodology): “The ATLAS9–ODFNEW models calculated by Castelli & Kurucz include improvements in the input physics, the update of the solar abundances from Anders & Grevesse (1989) to Grevesse & Sauval (1998) and the inclusion of a new molecular line lists for TiO and H2O.”
Constraining the thermally pulsing asymptotic giant branch phase with resolved stellar populations in the Large Magellanic Cloud (2019, methodology): “Model quantities are converted into the relevant photometry by means of extensive tables of bolometric corrections, derived from the stellar spectral libraries by Aringer et al. (2009) for C-rich stars, and Castelli & Kurucz (2003) plus Aringer et al. (2016) for O-rich stars.”
HIGH-RESOLUTION SPECTROSCOPY OF EXTREMELY METAL-POOR STARS FROM SDSS/SEGUE. I. ATMOSPHERIC PARAMETERS AND CHEMICAL COMPOSITIONS (2012, background): “The [Sr/Ba] ratio is very low ([Sr/Ba] = −2.1), suggesting the contribution of the s-process even at extremely low metallicity, which efficiently produces heavy elements due to the high ratio of neutrons to seed nuclei (e.g., Busso et al. 1999).”
THE ABUNDANCES OF NEUTRON-CAPTURE SPECIES IN THE VERY METAL-POOR GLOBULAR CLUSTER M15: A UNIFORM ANALYSIS OF RED GIANT BRANCH AND RED HORIZONTAL BRANCH STARS (2011, methodology): “To obtain preliminary estimates of Teff and log g for the M15 stars, photometric data from the aforementioned sources (Cudworth 2011; Buonanno et al. 1983(13); 2MASS) were employed as well as those data from Yanny et al. 1994(40).”
DETAILED CHEMICAL ABUNDANCES IN THE r-PROCESS-RICH ULTRA-FAINT DWARF GALAXY RETICULUM 2 (2016, methodology): “We interpolate model atmospheres from the onedimensional plane-parallel ATLAS9 grid of α-enhanced models (Castelli & Kurucz 2003).”
The vertical metallicity gradients of mono-age stellar populations in the Milky Way with the RAVE and Gaia data (2017, methodology): “For stars hotter than 10 000 K, Castelli & Kurucz (2003) model atmospheres are employed.”